JOYS: Unlocking accretion-rate diagnostics for high-mass protostars using JWST/MIRI HI lines

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Table 1.

JOYS source sample from millimetre observations.

Archive name	RA^a	Dec^a	D	$L_{bol}^{b}$ $Mathematical equation: $ L_{\mathrm{bol}}^{\,\,\,b} $$	Class	$M_{env}^{b}$ $Mathematical equation: $ M_{\mathrm{env}}^{\,\,\,b} $$	v_lsr	Mosaic	Other names	Ref.
	[J2000]	[J2000]	(kpc)	(L_⊙)		(M_⊙)	(km s⁻¹)
G28IRS2	18:42:51.99	−3:59:54.0	4.51	10 120	IRDC/HMPO	3288	77.7	1 × 1	G28P2	^3, 4, 12
G28P1	18:42:50.59	−4:03:16.3	4.51	682	IRDC	4276	80	2 × 2	–	^3, 4, 10
G28S	18:42:46.45	−4:04:15.2	4.51	364	IRDC	2296	78.4	1 × 1	C1-Sa	^{3, 4, 6, 7}
IRAS23385	23:40:54.49	61:10:27.4	4.90	3170	HMPO	220	−50.5	2 × 2	Mol160	^1, 2, 11
IRAS18089	18:11:51.24	−17:31:30.4	2.34	15 723^c	HMC	1100^c	34.1	2 × 1	G12.89+0.49	^{4, 5, 8, 9}
G31	18:47:34.33	−1:12:45.5	5.16	69 984	HMC	7889	97	1 × 1	−	^3, 4

Notes. 1: Beuther et al. (2023), 2: Molinari et al. (2008), 3: Wang et al. (2008), 4: Urquhart et al. (2018), 5: Xu et al. (2011), 6: Feng et al. (2016b), 7: Tan et al. (2016), 8: Cesaroni et al. (1994), 9: Beuther et al. (2002a), 10: Zhang et al. (2015), 11: Cesaroni et al. (2019), 12: Csengeri et al. (2016). ^a Coordinates of millimetre peak positions. ^b Properties were derived for emission that extends over larger spatial scales than those of the IR sources we report in Table 2 by factors of a few. ^c Distance corrected.

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